Micro-TDE CEJSN. A similar evolution to that of the double CEJSN might take place if instead of a NS the tight binary system is of a BH and a MS star when it enters the envelope of the RSG [1]}. The BH is several times the mass of the NS, and in many cases it will disrupt the MS star before it enters its intact envelope. The MS material forms a massive accretion disk around the BH, and the BH launches very energetic relativistic jets. The process by which a stellar BH disrupt a star and accretes its mass is termed a micro-tidal disruption event (micro-TDE; [2]}).
If the MS is very massive, the evolution might be through a BH-MS CEE, like for the NS. As well, if the MS is of low mass in the double CEJSN scenario, then the NS might disrupt the MS star before the systems enters a CEE. However, in most relevant cases a NS-MS tight binary system will enter a CEE and a BH-MS system will suffer a micro-TDE. Overall, the light curve of a micro-TDE CEJSN might be similar to that of double CEJSN event, but much more energetic and with relativistic jets.
One possible outcome of a BH accreting from the envelope of a RSG is the production of \(\approx 10^{15} {~\rm eV}\)  neutrinos [3]}.
